Pos(FRAPWS2016)045 fields field Dissipation field of Radio Pulsars

PoS(FRAPWS2016)045 fields http://pos.sissa.it/ field dissipation field of radio pulsars. field strength corresponds to average magnetic ∗ s – II – s ic are they magnetars? rophys st A Italy ), in ch . lermo ear 2016 [email protected] Res ay neutron star surface. SGR/AXP are connected with a magnetised stellar wind, induced by the bursting events near the librium layer of low mass neutron star is discussed. The losses of rotational energy, observed in The energy source, connected with the nuclear energy of superheavy nuclei stored in the nonequi- limit of the dipole magnetic were discovered, which don’t show any features of SGR, there are SGR/AXP in which an upper are indicated for this interpretation. Slow rotating radiopulsars with very high magnetic in a highly magnetized neutron star (magnetar) is analyzed. Some observational inconsistencies tron star. The model, where the source of the energy is connected with a magnetic (SGR/AXP) indicate to necessity of the energy source different from a rotational energy of a neu- The observational properties of Soft Gamma Repeaters and Anomalous X-ray Pulsars Speaker M ∗ ndello (Pa -28 Copyright owned by the author(s) under the terms of the Creative Commons rontier c F 23 Mo E-mail: ⃝ Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). SGR/AXP - G.S.Bisnovatyi-Kogan Space Research Institute, Profsoyuznaya str. 84/32,Research Moscow Nuclear 117997, University Russia, "MEPHI", and Kashirskoye National Shosse, 31, Moscow 115409, Russia PoS(FRAPWS2016)045 Gs 13 10 · 5 ÷ 11 10 · 4 G.S.Bisnovatyi-Kogan = ns B km, 10 = ns R , ⊙ R ) 10 1 ÷ 3 ( ∼ Gs (Lorimer 2005). R 13 10 · 5 Gs, at ÷ 100 11 ÷ 10 · 10 2 = = s ns B . Conservation of the magnetic flux gives an estimation of NS magnetic field as B , 2 ⊙ ) diagram for radiopulsars. Pulsars in binary systems with low-eccentricity orbits are encir- M ns ˙ P R 12 / - s ∼ P R ( > s B M Estimation of the NS magnetic field is obtained in radio pulsars by measurements of their Neutron stars (NS) are formed as a result of a collapse of the core of a massive star with a = ns cled, and in high-eccentricity orbits arewith supernova marked remnants, with from ellipses. Lorimer Stars (2005). show pulsars suspected to be connected Figure 1: rotational period and its time(Pacini derivative, 1967; in Goldreich the and model Julian oflowing 1969) a estimation Timing dipole observations radiation, of or single pulsar radiopulsars wind give the model fol- mass SGR/AXP - are they magnetars? 1. Introduction B (Ginzburg 1964). PoS(FRAPWS2016)045 = = P ergs, p rec L 43 keV was 10 ergs, 30 × 41 8 > . 10 kpc. Pulsations γ 6 E × > 10 6 ergs. The tail was s. There was not a p G.S.Bisnovatyi-Kogan ∼ 8 Q − 42 ergs, in the subsequent ≈ 39 10 44 P 10 × 10 7 ergs/s, × × 2 6 − 44 . 1 = 10 40 ≥ × 10 rec p 7 Q . × Q 3 5 > = seconds They produce "giant bursts", when p L 8 ergs/s, rec ÷ Q 41 2 2 orders of magnitude. Having a slow rotation, and keV: 10 6 × 15 ÷ 4 > 5 − γ E 40 was measured, being strongly variable. Accepting the distance ˙ 10 P × 2 year old SNR G42.8+0.6, situated at distance 4 = 10 p rec L ergs/s, and energy release in this object. ergs. The short recurrent bursts have peak luminosities in this region ˙ in the peak increase P 42 44 ergs, L ergs/s, the total energy release in the peak 10 10 43 45 × × 3 10 6 10 . 3 × − × 2 6 . = . 41 5 t 3 Detailed observations of this source are described by Mazets et al. (1999b,c), Kouveliotou It was discovered due to a giant burst of 5 March 1979, projected to the edge of the SNR First two Soft Gamma Repeaters (SGR) had been discovered by KONUS group in 1979. The It was suggested by Duncan and Thompson (1995), that the source of energy is their huge SGR are single neutron stars with periods 10 Q = ≥ t × p Q tail 3 et al. (1999), Woodslies et close al. to the (1999). less than The giant burst was observed 27 August, 1998. The source 2.2 SGR1900+14 N49 in LMC, and1982). described Accepting the by distance (Mazets 55 kpc et to al. LMC, the peak 1979b,c; luminosity in Golenetskii the et region al. 1979, Mazets et.al 10 kpc, this source had in the region 2.1 SGR0526-66 L observed about 3 minuteschance and to had measure regular pulsations with the period had been observed in thequiescence giant by RXTE burst, and as ASCA. well as in the X-ray emission observed in this source in first one, FXP 0520 -al. 66, 1979b,c; was Golenetskii discovered et afteronly al. the small 1979), famous recurrent see giant also bursts 5known Mazets had under March et.al names 1979 been (1982). SGR burst observed 0520 In (Mazets -identified (Mazets another et 66 as et source and a B1900+14 al. SGR repetitive 1900+14GRB070179 respectively. source 1979a). The was by third reported Laros SGR Now by 1806-20 et.al. Mazets thesethat was et this sources (1986a,b). al.(1981), source, are and The having itGRB, an first was similar unusually detection indicated to soft of by FXP0520 spectrum, this Mazets -forth can et source 66 known al. SRG1627-41, and belong as showing B1900+14. to giant (1982), a burst, ThisBATSE (Kouveliotou was separate suggestion et discovered al. was class in 1998a), completely 1998 of and almost confirmed. repetitive BeppoSAXobserved simultaneously (Feroci until The by et now al. in 4 1998). sources. The giant bursts had been small rotational energy, their observed averagethan 10 luminosity times, exceeds and rotational orders loss of of magnitude energy during more the giant outbursts. magnetic field, 2 orobjects 3 were order called magnetars. of a magnitude larger, then the average2. field SGR, in giant radiopulsars. bursts, and Such short GRB SGR/AXP - are they magnetars? The pulsars with a small magneticrecycling field by in accretion the in left a lower close angle binary. decrease see their Bisnovatyi-Kogan magnetic (2006). field during their luminosity PoS(FRAPWS2016)045 ˙ ˙ P P 11 ∼ − p Q 10 Gs. ergs/s, × 14 41 3 . 10 10 8 and variable ergs/s, × × = and average P 8 43 4 ˙ P P = 10 − B × G.S.Bisnovatyi-Kogan 40 8 10 years is much less than ∼ p × ergs/s, and magnetic field L 4 700 34 years, much smaller that the = = 10 s, and average ˙ keV: P p rec × correspond to 2 L 1500 5 / 47 ˙ . 15 . P P 3 ∼ 7 > p error. The peak luminosity in the burst = = γ = τ and p E σ P τ rot P ˙ E 3 s/s. The X-ray pulsar in the error box of this source was 10 − mJy, radiopulsar (Shitov 1999), with the same 10 years. These values of 50 × 4 5 = . 10 1 ergs/s is much higher, than rate of a loss of rotational energy, what means ergs. Periodicity in this source is not certain. max r − 36 s/s, the value in brackets gives 1 L 40 ergs/s in the region 25-60 keV, the X-ray luminosity in 2-10 keV band is 10 11 11 − 10 × − 41 2 10 × 10 10 ergs/s. The burst of December 27, 2004 in SGR 1806-20 was the greatest flare, 3 ergs/s is also much higher than the rate of the loss of rotational energy (for average × − Gs. The age of the pulsar estimated as × ∼ 33 5 − ) 35 35 14 4 10 . = p rec 39 ergs, no tail of the giant burst had been observed. 10 10 1 10 ˙ L ( P ≈ 10 × times brighter than ever. It was detected by many satellites: Swift, RHESSI, Konus-Wind, × 8 42 × . 2 s, 2 8 = 2 rot Here the giant burst was observed 18 June 1998, in addition to numerous soft recurrent bursts. Very strong luminosity of this outburst permitted to observe the signal, reflected from the moon The giant burst from this source was observed in December 27, 2004 (Palmer et al. 2005, 10 ˙ E ≈ = 100 = = 16 rec × ) , good corresponding to X-ray and gamma-ray observations. The values of x x . ˙ ˙ ˙ ∼ Coronas-F, Integral, HEND et al.. L P reaches Its position coincides with theobtained SNR for G337.0-0.1, a assuming possible periodicity 5.8 of kpc 6.7et distance. s, al. but Some giant evidences burst 1999a), did was contrary notobserved show to any with three periodic a signal other time (Mazets giant resolution burst 2 in ms SGR. at The photon following energy Q characteristics had been 2.4 SRG1627-41 by the HELICON instrument on thea board full of light the curve satellite of Coronas-F, what the permitted outburst to (Mazets reconstruct et al. 2005, Frederiks et al. 2007). Mazets et al. 2005,al. Frederiks et (1998b), Hurley al. et 2007). al.The (1999a). source Recurrent has bursts Connection a with had small the been butThe significant Galactic studied distance displacement radio by from to SNR Kouveliotou that G10.0-03 SNR et of was is thein found. non-thermal estimated this core as of object 14.5 this shows kpc. SNR. regular The pulsations X-ray with source observed a by period ASCA and RXTE 3 2.3 SGR1806-20 SGR/AXP - are they magnetars? 5 s/s. As in the previous case, it leads to the pulsar age discovered by Hurley et al.111 (1999b). MHz This as source was a discovered faint, also in radio band, at frequency that rotation cannot be aof source energy of comes energy from a in magnetic theseby field objects. Duncan annihilation, and and It Thompson such was objects (1992). suggested had been that called the as main magnetars source P correspond to the rate of a loss of rotationalthe estimated energy age of the closeL nearby SNR. Note that the observed X-ray luminosity of this object B age of SNR, estimated by is not constant, uniform setP of observations by RXTE gave much smaller and less definite value PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan erg (Golenetskii et al. 2005, jump was observed. ˙ 46 P E · 7 erg, in consistence with giant bursts of 45 E · 1 looks out surprising. for magnetic dipole losses, 4 4 . The first measurements have been done for SGR 1900 ˙ P and P , visible in Fig ˙ P . 4 - 2 The epoch folded pulse profile of SGR 1900 + 14 (2-20 keV) for the May 1998 RXTE observa- Despite the fact, that rotation energy losses are much smaller than the observed luminosity, The similarity between giant bursts in SGR, and short GRB was noticed by by Mazets et al. because it needs a considerableeffects. jump Contrary, in in the the magneticthat model field these of strength, losses pulsar strongly prohibited increase wind by during rotational self the energy giant induction losses burst, when it the looks quite reasonable, The pulse shape is changingthe from period. one The epoch big to jump another, in inducing errors in finding derivative of Figure 2: tions, from Kouveliotou et al. (1999). for estimation of the magneticpulsars, field based strength on measurements in of these objects used the same procedure as in radio 3. Estimations of the magneticin fields SGR/AXP (1999), Bisnovatyi-Kogan (1999). The experimentinterpreted KONUS-WIND as had giant observed bursts two of short SGR. The GRB, 1 first February, 2007. one, GRB070201, The was energy observed of in the M31 burst (Andromeda), is equal to SGR/AXP - are they magnetars? 2.5 SRG giant bursts in other galaxies other SGR Mazets et al.M81, (2008). 3 The November second 2005. short burst, TheFrederiks GRB051103, energy et was al. of observed the 2007). in the burst galaxy is equal to + 14, in different epochs by measurementspresented of in satellites RXTE Figs. and ASCA (Kouveliotou et al. 1999), PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 5 ]. The time is given in Modified Julian Days (MJDs), from Kouveliotou et al. 30 The evolution of "Period derivative" versus time since the first period measurement of SGR The epoch folded pulse profile of SGR 1900 + 14 (2-20 keV) for the August 28, 1998 RXTE Figure 4: (1999) 1900+14 with ASCA in [ Figure 3: observation. The plot is exhibiting two phase cycles, from Kouveliotou et al. (1999). SGR/AXP - are they magnetars? PoS(FRAPWS2016)045 ˙ I. ˘ A ˇ T1744 ˘ A ˇ T0130: A ˘ A , and therefore ˙ P ˘ AIJmagnetarsâ G.S.Bisnovatyi-Kogan ˙ I), these results suggest ˘ G; G; A 13 13 10 10 G. · · 1 5 13 ˇ T 6127 and PSR J1814 â . . ˘ 4 5 A 10 · ˇ = = T1744 has spin parameters similar to 4 ˘ . A B B 9 G. ˘ AIJ magnetars â s/s, s/s, 13 12 13 10 s/s, B= · − − 4 . 12 6 10 10 7 · · − 0 4 = . . 10 4 7 · B 3 . = = 1 ˙ ˙ P P = ˙ P SGR/AXP J1550-5418 (1E 1547.0-5408) was visible in radio band, showing pulsations with a 4. PSR J1718 - 37184, P= 3.4 s , 3. PSR J1847 - 0130, P=6.7 s, Soon after this discovery, several other radio pulsars were found, where also 1. PSR J1119 - 6127, P2. = PSR 0.407 J1814 s, - 1744, P = 3.975 s, Radio pulsars are rotating neutron stars that emit beams of radio waves from regions above the anomalous X-ray pulsar (AXP)AXPs IE are 2259 isolated, + high 586, magneticthat but field their shows neutron unusual no stars attributes discernible (â magnetic are X-ray fields." unlikely emission. to If be merely a consequence of their very high inferred show apparently normal radio emission inpredict a that regime no of emission magnetic field should strength occur. where Also, some models PSR J1814 â RADIO PULSAR WITH MAGNETAR SPIN CHARACTERISTICS", thatpulsar prove "The that properties inferred of dipolar this magnetic fieldthe strength and unusual period high-energy cannot properties alone be of responsiblethe the for possible magnetars relationship and between create these new two challenges manifestations of for young understanding neutron stars." The lack of AXP-likeemission X-ray from emission the from AXPs) these createsthe relationship radio new between challenges pulsars these for classes (and understanding of the apparently pulsar young non-detection emission neutron of physics stars." radio and 5. SGR/AXP with low magnetic fields and moderate rotation It was noted in thethe paper anomalous of X-ray McLaughlin pulsars et (AXPs), al. which (2004), growing that evidence "These suggests fields are are â similar to those of It was noted in the paper of McLaughlin et al. (2003), with the title "PSR J1847â magnetic field strength was measured (Manchesteral. et 2003,2004). al. These 2001, pulsars Camilo include: et al. 2000, McLaughlin et It was noted by Camilo et al. (2000), that "Both PSR J1119 â their magnetic poles. Popularpositron pair theories production, with of the potential the responsiblerelated for emission accelerating to mechanism the the particles spin require being period. inversely continuous Pairthe electron- production models will predict stop that when radio the emissionthe potential will magnetic drops field cease strength below when and a the configuration. threshold, period It so J2144-3933 was exceeds has shown a by a value Young period et that of al. depends 8.51s, (1999a,b) on whichunder that the is the usual pulsar by model far assumptions, the based longest on of thepulsar neutron-star any should equations known not of radio state, be pulsar. this emitting Moreover, slowly a rotating current radio theories beam. of Therefore radio either theSGR/AXP emission model objects, must assumptions but be are this wrong, revised. pulsar or radio does The pulsar. not period show 8.51 any violent second behaviour, is and characteristic behave for like ordinary SGR/AXP - are they magnetars? 4. Radiopulsars with very highfields magnetic and slow rotation PoS(FRAPWS2016)045 ) B 4 G, 15 Gauss, . 10 s 12 4 ÷ 10 14 ∼ · 5 10 . 7 G.S.Bisnovatyi-Kogan , as well as in the pulse ˙ P ), gives a strong indication that 5 keV (Kaneko et al., 2010). The INTEGRAL 7 110 observed in the giant burst of PSR1900+14 (Fig. ∼ ˙ P in several SGR (McGill 2014), seems to support this ˙ P and P keV, showing a periodicity with P=2.1s (Kuiper et al. 2009). This object values similar to radio pulsars (Section ), detection of SGR with a small rotational period and low magnetic field, ˙ 4 P 150 are not justified, because magnetic stellar wind could be the main mechanism give the values characteristic for usual radiopulsars, when there is a presence of ÷ ˙ and P s (Camilo et al. 2007). The pulsations with the same period have been observed ˙ P 20 P ) have not been seen in the radio pulsars. In the fall-back accretion model of SGR 069 3 and . , 2 2 P = P When the energy density of the magnetic field is much larger that that of matter, as expected Subsequent observations of In the paper of Duncan and Thompson (1992) was claimed, that dynamo mechanism in the A low-magnetic-field SGR0418+5729 was detected by Fermi gamma-ray burst detector (Rea called magnetars. These magnetars could bea responsible for plausible cosmological model GRB, for and SGR. may In represent between the magnetars subsequent and paper (Duncan SGR and wasSGRs, Thompson developed and 1995) the in the energetic connection more 1979 March details. 5fields burst, much The based stronger authors on than the presented those existence of a of ordinary neutron model pulsars. stars for with magnetic estimations using form (Figs. in the surface layersThe of observations of the radio magnetar, pulsars, the showingslow no rotation instability traces (Section should of bursts, be withestimated suppressed magnetar from magnetic by fields magnetic and forces. inferred dipolar magnetic field strength and period cannotenergy alone properties be of responsible for SGR/AXP. the Therefore, unusual another high- for characteristic a parameter violent should behaviour of be SGR/AXP. responsible The unusually low mass of the neutron star was suggested by of angular momentum losses. The jump in model. However, when the rotation energy losses are much less than observed X-ray luminosity, (Chatterjee et al. 2000,field Alpar using 2001, Trümper et al. 2010, 2013) the estimations of the magnetic new born rapidly rotating star may generate NS with a very strong magnetic field is plausibly explained by ajump corresponding in the increase dipole of magnetic field the strength magnetic is stellar hardly possible. wind The power, jumps while in the a large scale magnetic field in the fall back accretion disk (Bisnovatyi-Kogan and Ikhsanov 2014). is the only SGR/AXP with a relatively low period, all previous has periods exceeding 6. The Magnetar Model et al. 2010).detected after This it emitted soft bursts gamma similar"X-ray to repeater observations those with of show magnetars. that low It its magnetic was dipolar noted field by magnetic SGR0418+5729 Rea field et was cannot al. recently be (2010) that greater than SGR/AXP - are they magnetars? period detected pulsed soft gamma-rays fromthe SGR/AXP energy 1E1547.0-5408 band during its Jan-2009 outburst, in well in the range ofnot ordinary necessarily radio required pulsars, for magnetar-like implying activity". that a high surface dipolar magnetic field is first only in the soft Xstatistics ray of band photons by was XMM-Newton not (HalpernOctober et enough and al. in for 2009 2008). detection January In of andof the pulsations. March, 2.1s hard observed was X In by ray clearly Fermi the region visible gamma-ray strong burst up outbursts monitor, to in the the period 2008 energy PoS(FRAPWS2016)045 (6.2) (6.3) (6.4) (6.5) (6.6) (6.7) (6.8) (6.1) , which energy w G.S.Bisnovatyi-Kogan as (Weber and Davis . J 3 ) are the most important, ) . c w 6.1 . 6 A the density is equal to ( 2 r L Ω is rate of the loss of rotational ˙ π µ is equal to the magnetic energy M 8 rot = rot w wind ˙ ˙ E is the magnetic dipole moment of E F E = 3 ∗ 4 3 PRS ˙ r . J s BA B = 2 E . ˙ 3 µ , , Mw 6 = ∗ . ) L 2 A w , 6 ∗ . r ˙ 2 c ˙ µ w Ω = 2 A r 2 = Mr ˙ 3 r 3 Ω Ω 2 ( 4 A ˙ 2 ˙ ˙ π r ˙ Ω Ic Ω wr Mw I M 2 Ω M 8 2 3 / π ˙ 2 3 Ω 8 9 4 Ω 2 I 4 , = = Ω = , where = I = BA ˙ = 3 Mw wA E ˙ r we obtain its value as E 2 PSR ρ E / 4 3 , and when the wind losses ( wind A ˙ B 2 wind = µ J r Ω B = , I , 6 wA ∗ = 2 A r w = E ˙ 4 B ˙ 3 M ˙ Ω J wr 3 c M Ω π c 2 s Ω I 4 2 B 3 = = = A L ρ 2 PSR 2 wind . In a stationary wind with a mass loss rate 2 B . We consider the wind with a constant outflowing velocity B ) w ) the magnetic field if the dipole radiation losses are the most important π ρ 8 5 ( . 6.6 / 0 2 B = w is the the energy flux carried away by the wind, and = E B is Alfven radius, where the energy density of the wind E wind A F r A magnetic stellar wind carries away the stellar angular momentum the star. At the Alfven radius we have Here The ratio of these two values is written as The angular momentum and energy losses byradiopulsars the are dipole written radiation which as are (Pacini main 1967) losses in ordinary We obtain from ( The angular momentum of the star density From the definition of the Alfven radius we obtain the value of stellar magnetic field as energy. For estimation of the energy flux carried away by the wind could be used the average For the dipole stellar field we have here 6.1 Angular momentum losses by a magnetized stellar wind SGR/AXP - are they magnetars? Bisnovatyi-Kogan (2012), Bisnovatyi-Kogan and IkhsanovSGR/AXP (2014) neuron as stars from a the parameter, majority of distinguishing neutron stars in radio pulsars and close X-ray binaries. 1967) density is PoS(FRAPWS2016)045 ) < 3 / P c (6.9) ( < 1 ≈ P , ∗ 1 r GM 2 ρ < √ ρ = < f f ; in region II we have G.S.Bisnovatyi-Kogan 2 v , from Bisnovatyi-Kogan ρ nb separates region I, where ) Q ρ ( nb > f e Q n ε Q we have and ⊙ ) . The line with the attached shading M β T 8 ( ε . determines the boundaries for the values 0 nb Gs respectively. While the mechanical > Q ≤ f e 13 . abcd ε γ M 10 x , rot · ˙ L E nb 6 Q , 36 9 14 < = n . In region I we have 10 Q · 7 max 2 PSR 2 wind , and the wind velocity is of the order of the free fall . β γ B 1 B ε x , ) we obtain for the magnetic fields of SGR 0526-66, SGR L 13 6.9 10 , these values of the magnetic field are suppose to be the upper γ x < ... < L 2 -decay. The shaded region β ε α < 1 β ε km, and ; n 15 Q ; and in region III we have = β − ∗ ε r p , < Q ⊙ f e = M ε The formation of chemical composition at the stage of limiting equilibrium. The thick line 6 β , . ε -ray luminosity of SGR/AXP 0 nb γ 0 defines the boundary of the region of existence of nuclei, the line Q = It was shown by Bisnovatyi-Kogan and Chechetkin (1974), that in the neutron star crust full = < M , with n n 2 P of (A,Z) with a limited equilibrium situation, at given values of loss of the energy could exceed photodisintegration of neutrons is impossibleconstant from regions II andQ III. The dashed linesindicates indicate a region a of level fission of and The non-equilibrium layer is formed in the region of densities and pressure Figure 5: Q at 1806-20, SGR 1900+14 the values thermodynamic equilibrium is not reached,neutron and star cooling, a see non-equilibrium also layer Bisnovatyi-Kogan (2001). is formed there during a velocity of the neutron star. For low mass neutron star limit if the magnetic field of these SGR. 7. Model of nuclear explosion Using data from McGill(2014) and ( SGR/AXP - are they magnetars? X and and Chechetkin (1974). PoS(FRAPWS2016)045 , 39 ⊙ M 10 ) 8 − . 0 38 . Namely, ÷ 10 4 4 . 0 ( , 3 ⊙ 3 G.S.Bisnovatyi-Kogan . cm M / 4 cm g / − g 10 10 12 10 ≃ · 10 5 g . in cgs units . ≃ 1 6 29 3 30 erg erg) the mass of the ejected material ≃ -ray bursts of the order of 10 10 48 3 γ cm · · 41 / 2 10 1 g cm . 10 e / 2 · ≃ ≈ g µ 2 ) ) = e 1 1 11 P 2 µ ∼ P 9 P 10 − − · 2 10 10 2 ps. The schematic picture of the nuclear explosion 7 · , P P . ( ( 8 2 1 . . 17 3 100 ≃ 0 3 10 ≃ ∼ ≃ · 3 ) ) was considered, where the nonequilibrium layer is relatively 4 1 ) ) P ≃ in cgs units ⊙ 511 33 . − nl 8 M 511 0 27 2 . E 2 P 0 , and the energy release in the nuclear reaction of fission is about ( 10 ( 4 6 ∼ · ( 4 ( g). This leads to energies of the 6 1 R ≃ 10 . e π 7 e 21 GM 10 µ 4 e µ = 10 µ ≃ = 1 ∼ 2 P ≃ nl ρ 1 M ρ erg/g. Soon after discovery of gamma ray bursts the model of nuclear explosion was 2 c 3 − It was suggested by Bisnovatyi-Kogan (2012,2015), Bisnovatyi-Kogan and Ikhsanov (2014), 10 · that the property, making thein SGR radio neutron pulsars, star single so andnot different binary the from magnetic X much field ray more strength, sources,it numerous see is was of Camilo suggested connected them (2000), that with the McLaughlin the neutron (2003), value stars and of in Section their SRG/AXP mass, have anomalously but low mass, of the matter from the non-equilibriumCosmological layer origin is of presented GRB, in and Fig. identificationas of a SGR/AXP group lead of to non-stationary sources considerableal. inside revision Galaxy (1975). of It the becomes older clear model,produce that presented SGR bursts by represent much a Bisnovatyi-Kogan more very et powerful, rareCrab than and nebula it very pulsar. special was Besides, type thought the of before SGRbe objects, from are applied, which the because comparison only the with sources energy quakes for releasethe in which in non-equilibrium the the layer. cosmological nuclear GRB explosions could highly exceed the energy store in 5 suggested (Bisnovatyi-Kogan et al. 1975), inlower which densities the during non-equilibrium a layer starquake. matterthe is At Galaxy, brought the and to beginning the GRB outburst have wasto been connected those considered with observed as period objects in jumps inside theneutron in Crab stars the may nebula neutron be pulsar. related star to rotation It thekinetic similar observed was energy jumps of suggested of the periods that: of filaments pulsars. of "Ejection From the of the Crab observed matter Nebula gain from ( of the erg, which agrees fully with observationsdetailed at the model mean of distance up the to strongconsidered the by sources 5 Bisnovatyi-Kogan 0.25 and March kpc". Chechetkin 1979 A (1981). more burst, ItNS was inside now identified the classified with galactic an as disk, explosion at SGR on a the 0526-66 distance in LMC, was Here a neutron star of a large The mass of the non-equilibrium layer is defined as (Bisnovatyi-Kogan and Chechetkin 1974) and the energy stored in this non-equilibrium layer is estimated as thin, and its mass,nuclei and in the the non-equilibrium energy layer store areone overabundant are with electron estimated neutrons, is so in taken the the as number of approximation nucleons of per a flat layer. The SGR/AXP - are they magnetars? may be estimated as ( PoS(FRAPWS2016)045 = p m was belonged ⊙ M 4 − G.S.Bisnovatyi-Kogan 10 ≈ nl M % probability. It was suggested 4 . 95 times larger. The energy store reaches 7 ∼ with a ⊙ M ) 11 51 . 0 − , (see Bethe and Johnson 1975, Malone et al. 1975). For 58 ⊙ . giant bursts. 0 M 2 (+ 1000 ∼ 00 . ∼ 2 = e m (Ferdman et al. 2014). The violent behaviour of the low-mass NS may be , ) ⊙ ⊙ M M the calculated mass of the non-equilibrium layer 23 7 . 58 . the mass of the non-equilibrium layer is 1 0 ⊙ ≥ − , M The schematic picture of non-equilibrium layer in the neutron star: a) in a quiescent stage; b) after 1. SGR are highly active, slowly rotating neutron stars. 51 45 . . . In Sect. erg, what is enough for 0 0 7 49 The observational evidences for existence of neutron stars with masses, less than the Chan- (+ = 10 ns 72 . by Bisnovatyi-Kogan and Ikhsanovscenario (2014) of that the low off-center mass explosionvestigation (Branch neutron is and needed stars Nomoto to could 1986), prove be butby it. Bisnovatyi-Kogan more formed and X-ray detailed Ikhsanov in radiation numerical (2014) the as of in- poloidal a SGR/AXP magnetic fall in field, back quiescent accretion what states from could the wasmixing also disk in explained be with the a a neutron trigger large star for scale envelope,layer. development and of nuclear instability, explosion leading of to the the matter from the non-equilibrium to the neutron star with the mass 0 8. Conclusions drasekhar white dwarf massof limit the have binary been pulsar obtained system by Janssen J1518-4904 et indicated al. the masses (2008). of the Observations components to be connected with much thicker and moreback massive highly non-equilibrium magnetized layer, and accretion accretion disk from could(Bisnovatyi-Kogan the trigger and fall- the Ikhsanov instability, leading 2014). to The outburstsin explosions NS a radius flat is approximation increasingMore the with accurate mass mass estimations rather of have been slowly, non-equilibrium obtained so in layer from Fig. calculations is of inversely neutron proportional star models, to presented the mass. starquake and nuclear explosion, from Bisnovatyi-Kogan (1990). M ∼ Figure 6: compared to the well measured masseshave in masses binary systems of two neutron stars, where neutron stars SGR/AXP - are they magnetars? PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 12 ] was used to construct the model of the neutron star, with the boundaries of 54 , 2 Dependence of the mass of the non-equilibrium layer on the neutron-star mass. The lines show 5. The upper boundary of the magnetic fields in 3 most famous SGR, measured by the average 6. Magnetar model of SGR, in which the energy of the observed bursts is provided by magnetic 3. The mass and the energy4. store in NL The increase properties rapidly with of decreasing pulsar of NS with mass. high magnetic fields prove that inferred dipolar magnetic 2. Nonequilibrium layer (NL) is formed in the neutron star crust, during NS cooling, or during luminosity is about one order of magnitude lower than the values obtained using the pulsar-like γ x L field annihilation, seems to bemagnetic not field, relevant. and of Observations a of low-field "magnetar", quietrapid is radiopulsars growth the of most with important rotational a indication periods, "magnetar" to what that is conclusion. a A favorite argument for a "magnetar" origin, is naturally field strength and periodSGR/AXP. cannot The NL alone in be low mass responsible NS for may be the responsible unusual for bursts high-energy and properties explosions in of them. energy losses of the rotational energy of the neutron star. accretion onto it. ItSGR. may be important for NS cooling, glitches, and explosions connected with Figure 7: the top and bottom boundaries ofthe the equilibrium layer matter mass [ measured fromthe the layer stellar specified surface. by The the equationlayer, densities. of but Using state should a of not non-equilibrium fundamentally equationcalculated of change and state the prepared will by values increase S.O. given Tarasov. the in mass the of figure, the from Bisnovatyi-Kogan (2012), SGR/AXP - are they magnetars? PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 13 Camilo F., Kaspi V. M., Lyne A.G.,Crawford Manchester F. (2000) R.N., Discovery Bell of J.F., D’Amico Two High N., Magnetic McKay Field N.P.F., Radio Pulsars. ApJ 541: 367-373 Branch D., Nomoto K. (1986) Supernovaedwarfs? of Astron. Type and Ib Astrophys. as 164: off-center explosions L13-L15 in accreting white Bisnovatyi-Kogan G.S., Chechetkin V.M. (1974) Nucleosynthesis inChemical Supernova Composition Outbursts of and the the Envelopes of Neutron Stars.Bisnovatyi-Kogan ApSS G.S., 26: Chechetkin 25-46 V.M. (1981) Gamma-Ray BurstsInherent as Activity a of Manifestation Neutron of Stars. the Sov. Astron. 58:Bisnovatyi-Kogan 561-568 G.S., Imshennik V.S., Nadyozhin D.K., Chechetkin,gamma-ray V.M. emission (1975) from Pulsed neutron and collapsing stars andBisnovatyi-Kogan supernovae. G.S. ApSS and 35: Ikhsanov 23-41 N.R. (2014)Astronomy A Reports new 58: look 217-227 at anomalous X-ray Pulsars. Bisnovatyi-Kogan G.S. (2012) Gamma ray bursts,Proceedings their of afterglows, the and Workshop soft "Gamma-Ray gamma Bursts: repeaters.Environment" Probing Moscow, In 13 the - Science, 15 Progenitors June andhttp://www.exul.ru/workshop2012/Proceedings2012.pdf 2012, their pp.1-4; Bisnovatyi-Kogan G.S. (2015) SGR/AXP - arevol. they 29, magnetars?. No. Astron. 2 Astrophys. Transactions; Bisnovatyi-Kogan G.S. (2017) Young neutron stars withX-ray soft pulsar. in gamma "Handbook ray of emission Supernovae", andPublishing A.W. anomalous Alsabti, P. Murdin (Eds.) Springer International Bisnovatyi-Kogan G.S. (2006) Binary and recycledPhysics pulsars: Uspekhi 30 49: years 53-67 after observational discovery. Bethe H.A., Johnson M.B. (1974) DensePhysics baryon A230: matter l-58 calculations with realistic potentials. Nuclear Bisnovatyi-Kogan G.S. (1992) Gamma-ray bursts fromTaos nuclear (USA) fission "Gamma-ray in bursts neutron - stars. Observations, In: analyses and ProcBisnovatyi-Kogan theories" Conf. G.S. (A93-20206 (1999) 06-90), Magnetic pp. fields 89-98 ofastro-ph/9911275 neutron (Proc. stars: Vulcano very Workshop 1999, low Memorie and(2002) della very 73: Societa high. Astronomica 318-329) Italiana Bisnovatyi-Kogan G.S. (2001) Stellar Physics. Vol.1. FundamentalSpringer concepts and stellar equilibrium, Alpar M.A. (2001) On Young NeutronFields. Stars ApJ as 554: Propellers 1245-1254 and Accretors with Conventional Magnetic The work was supported by the Russian Scientific Foundation Grant No. 15-12-30016 Acknowledgments [8] [9] [7] [4] [5] [6] [2] [3] [1] [14] [15] [12] [13] [10] [11] References SGR/AXP - are they magnetars? explained by action of thesuppresses magnetic convection, stellar which wind. is needed Besides, in the all high annihilation pressure models. of the magnetic field PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 14 ˘ a C. (1995) The soft gamma repeaters as very strongly magnetized ˘ a R.C., Thompson Kouveliotou C., Kippen M., Woods P., RichardsonPreviously G., Unknown Connaughton Soft V. Gamma-ray (1998a) Repeater BATSE Discovery SGR1627-41. of The Astronomer’s Telegram No. 29 Hurley K., Li P., Kouveliotou C.,Luginbuhl Murakami C., T., Ando Yoshida A., M., Smith Strohmayer I. T.,SGR van (1999b) 1900+14. Paradijs ASCA J., ApJ Discovery Vrba 510: of F., an L111-L114 X-Ray Pulsar inJanssen the G.H., Error Stappers Box B.W., of Kramer M.,Multi-telescope Nice timing D.J., of Jessner PSR A., J1518+4904. Cognard Astronomy I., and Purver Astrophysics M.B.Kaneko 490: (2008) Y., 753-761 Goegues E., Kouveliotou C., GranotFinger J., M.H., Ramirez-Ruiz Gehrels E., N., van Pe’er der A.,Woods Horst P.M. van (2010) A.J., der Magnetar Watts Klis A.L., Twists: M., Fermi/Gamma-Ray von BurstJ1550-5418. Kienlin Monitor ApJ A., Detection 710: Wachter of S., 1335-1342 SGR Wilson-Hodge C.A., Hurley K., Kouveliotou C., Cline T.,Where Mazets is E., SGR Golenetskii 1806-20? S., Frederiks ApJ D., 523: van L37-L40 Paradijs J. (1999a) Golenetskii S.V., Mazets E.P., Il’inskii V.N., Gur’yanthe Yu.A. (1979) flaring Recurrent source gamma-ray FXP bursts 0520 from - 66. Soviet AstronomyGoldreich Letters P., Julian 5: W.H. (1969) 340-342 Pulsar Electrodynamics. ApJ 157:Golenetskii 869-880 et al. (2005) IPN triangulationGCN and 4197 Konus spectrum of the bright short/hard GRB051103. Halpern J.P., Gotthelf E.V., Reynolds J., RansomAnomalous S.M., X-Ray and Pulsar Camilo 1E F. 1547.0-5408. (2008) ApJ Outburst 676: of 1178-1183 the 2 s Ginzburg V.L. (1964) The Magnetic FieldsPhysics of Doklady Collapsing 9: Masses and 329-334 the Nature of Superstars. Soviet Feroci M., Costa E., Amati L.,SGR1627-41, Piro BeppoSAX-GRBM L., detections. Martino GRB B., Coordinates di Network, Ciolo 111 L., ColettaFrederiks A., D.D., Frontera, Golenetskii F. S.V., (1998) Palshin V.D., Aptekar’E.P., Cline R.L., T.L. Ilyinskii (2007) V.N., Oleinik Giant F.P., flare Mazets inAstronomy SGR Letters 1806-20 33: and 1-18 its Compton reflection fromFrederiks the D.D., Moon. Palshin V.D., Aptekar’ R.L.,the Golenetskii possibility S.V., Cline of T.L., identifying and the Mazets shortrepeater E.P. (2007) hard in On burst the GRB M81 051103 group with of a galaxies. giant Astron. flare Letters from 33: a 19-24 soft gamma Ferdman R.D., Stairs I.H., Kramer M.,neutron et star al. companion. (2014) MNRAS PSR 443: J1756-2251: 2183-2196 a pulsar with a low-mass Camilo F., Ransom S.M., Halpern J.P., ReynoldsMagnetar J. with (2007) a 1E Rotation 1547.0-5408: Period of A 2 Radio-emitting Seconds.Chatterjee ApJ P., Lett. Hernquist 666: L., L93-L96 Narayan R.ApJ (2000) 534: An 373-379 Accretion Model for Anomalous X-Ray Pulsars. Duncan R.C., Thompson C. (1992) FormationImplications of for very gamma-ray strongly bursts. magnetized ApJ neutron Lett. stars 392: - L9-L13 Duncan neutron stars - I. Radiative mechanism for outbursts. MNRAS 275: 255-300 [33] [31] [32] [28] [29] [30] [26] [27] [24] [25] [22] [23] [20] [21] [17] [18] [19] SGR/AXP - are they magnetars? [16] PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 15 -ray repeater SGR1806 - 20. Nature, 393: 235-237 γ Mazets E.P., Cline T.L., Aptekar’ R.L., ButterworthV.N., Pal’shin P., V.D. Frederiks (1999c) D.D., Activity Golenetskii of S.V., the Il’inskii Konus-Wind soft observations: gamma 2. repeater The SGR giant 1900 August + 27 14 outburst. in Astronomy 1998 Letters from 25: 635-648 Mazets E. P., Golenetskii S. V., Guryanthe Yu, distinct A. class & of Ilyinski short V. N. gamma173-189 (1982) bursts The Are 5 they March of 1979 the event same and origin. Astrophys.Mazets Space E.P., Sci. Aptekar’ 84: R.L., Butterworth P., ClineIl’inskii T.L., V.N. (1999a) Frederiks Unusual D.D., Burst Golenetskii Emission S.V., HurleyApJ from K., Lett. the 519: New Soft L151-L153 Gamma Repeater SGR 1627-41. Mazets E.P., Cline T.L., Aptekar’ R.L., ButterworthV.N., Pal’shin P., V.D. Frederiks (1999b) D.D., Activity Golenetskii of S.V., the Il’inskii Konus-Wind soft observations: gamma 1. repeater Short SGR recurrent 1900 bursts. + Astronomy 14 Letters in 25: 1998 628-634 from Mazets E.P., Golenetskii S.V., Il’Inskii V.N., Panov V.N.,Sokolova Aptekar’ Z.Ya., R.L., Kharitonova T.V. Gur’yan (1979b) Yu.A., A Sokolov flaring I.A., Letters, x-ray 5: pulsar in 163-166 Dorado. Soviet Astronomy Mazets E.P., Golentskii S.V., Ilinskii V.N., Aptekar’flaring R.L., X-ray Guryan pulsar Iu.A. in (1979c) Dorado. Observations Nature, of 282: a 587-589 Mazets E.P., Golenetskii S.V., Il’inskii V.N., PanovSokolov V. N.; I.A., Aptekar Sokolova R.L., Z.Ya., Kharitonova Gur’yan T.V., Dyatchkov Y.A., Proskura A.V.,cosmic Khavenson M.P., gamma-ray N.G. bursts (1981) from Catalog the of KONUS experiment data. Ap. Space Sci. 80: 3-143 Mazets E.P., Golenetskii S.V., Gur’yan Yu.A. (1979a)B1900+14. Soft Soviet gamma-ray Astronomy bursts Letters from 5: the 343-344 source Laros J.G., Fenimore E.E., Klebesadel R.W.,Gamma Kane Repeater S.R. (SGR) (1986a) GB790107. Statistical Bulletin Properties of of the the American Soft AstronomicalLaros Society J.G., 18: Fenimore 928 E.E., Fikani M.M.,burst Klebesadel GB790107. R Nature W., 322: Barat 152-153 C. (1986b) The soft gamma-ray Lorimer D.R. (2005) Binary and Millisecondhttp://www.livingreviews.org/lrr-2005-7 Pulsars. Living Reviews in Relativity 8: 7-82; Manchester R.N., Lyne A.G., Camilo F.,F., Bell Stairs J.F., I.H., Kaspi Possenti V A., M., Kramer D’AmicoI. M., N., Observing Sheppard McKay and D.C. N.P.F., Crawford data (2001) analysis The systems, Parkes discovery multi-beam and pulsar timing survey of - 100 pulsars. MNRAS 328: 17-35 Kouveliotou C., Dieters S., Strohmayer T.,Kommers van J., Paradijs Smith J., I., Fishman Frail G.J., D., Meeganfield Murakami C.A., in T. Hurley the (1998b) K., soft An X-ray pulsar with a superstrongKouveliotou magnetic C., Strohmayer T., Hurley K.,Thompson van C., Paradijs Duncan J., R.C. Finger (1999) M.H., Discovery DietersRepeater of S., SGR a Woods 1900+14. P., Magnetar ApJ Associated Lett. with 510: the L115-L118 Soft Gamma Kuiper L., den Hartog P. R.,gamma-rays Hermsen from W. (2009) SGR/AXP The 1E1547.0-5408 INTEGRAL during detection itsTelegram of 1921, JAN-2009 outburst. pulsed 01/2009 The soft Astronomer’s [48] [46] [47] [44] [45] [43] [41] [42] [39] [40] [37] [38] [35] [36] SGR/AXP - are they magnetars? [34] PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 16 Young M.D., Manchester R.N., Johnston S.radio (1999b) pulsar Ha, with ha, an ha, 8.5-s ha, period stayingBeyond, challenges ASP alive, emission staying Conference models. alive: Series, In: Vol. A 202 Pulsar pp.185-188;in Astronomy Proc. Bonn, - of Germany, 30 2000 the August and 177th - Colloquium 3 of September the 1999; IAU held eds. M. Kramer, N. Wex, and R. Wielebinski Trümper J.E., Zezas A. , ErtanX-Ray U., Pulsar Kylafis 4U N.D. 0142+61. (2013) ApJ An 764: Accretion 49-58 Model forWeber E.J. the and Anomalous Davis L.J. (1967) The Angular MomentumWoods P.M., of Kouveliotou the C., Solar van Paradijs Wind. ApJ J.,Strohmayer, 148: Finger T., Swank, M.H., 217-227 J., Thompson, Murakami, C., T. Duncan, (1999)SGR R.C., Variable 1900+14 Hurley, Spin-Down K., and in Correlations the with Soft Burst Gamma Activity. Repeater ApJYoung 524: M.D., L55-L58 Manchester R.N., Johnston S.challenges (1999a) emission A models. radio Nature pulsar 400: with 848-849 an 8.5-second period that Trümper J.E., Dennerl1 K., Kylafis N.D.,characteristics Ertan of U., the Zezas anomalous A. X-ray (2010) pulsar The 4U spectral 0142+61. and Astron. beaming and Astrophys. 518: A46-A51 Rea N., Esposito P., Turolla R.,Goegeus Israel, E., G.L., Kouveliotou Zane C. S.; (2010) Stella A L.;944-946 Low-Magnetic-Field Mereghetti Soft S., Gamma Tiengo Repeater. A., Science Goetz 330: D., Shitov Yu.P. (1999) SGR 1900+14 = PSR J1907+0919. IAU Circ No. 7110, Feb. 17 Pacini F. (1967) Energy Emission from a Neutron Star.Palmer Nature D.M., 216: Barthelmy S., 567-568 Gehrels N.,R.A.M.J., Kippen, Woods, R. P. M., M.; Granot Cayton J., T., Lyubarsky KouveliotouCummings Y.E., C., J., Ramirez-Ruiz Eichler Fenimore E., D., E.E., Barbier Wijers Finger L., M.H., ChesterNousek Gaensler M., J.A., B.M., Parsons Hullinger A., D., Patel Krimm S.,gamma-ray H., Sakamoto flare Markwardt T., from C.B., Sato the G., magnetar Suzuki SGR M., 1806 Tueller - J. 20. (2005) Nature, A 434: giant 1107-1109 McLaughlin M.A., Lorimer D.R., Lyne AManchester G., R.N., Kramer Hobbs M., G., Faulkner Camilo A.J., F.,Magnetar Kaspi Possenti Fields. V.M., A., Stairs Young D’Amico Neutron I.H., N. Stars (2004) andpart Two Their Radio of Environments, Pulsars the IAU with Symposium IAU General no. Assembly, 218,and 14-17 held Bryan July, as 2003 M. in Gaensler. San Sydney, Australia. Francisco, Edited CA: by AstronomicalMalone Fernando Society R.C., Camilo of Johnson the M.B., Pacific, Bethe 2004., H.A. pp.255-256 equations (1975) of Neutron state. star ApJ models 199: with 741-748 realistic high-density McLaughlin M.A., Stairs I.H., Kaspi V.M.,Camilo Lorimer F., D.R., Hobbs Kramer G., M., Possenti Lyne A., A.G.,Pulsar D’Amico Manchester with N., R.N., Magnetar Faulkner Spin A.J.(2003) Characteristics. PSR ApJ J1847-0130: Lett. A 59l: Radio L135-L138 Mazets E.P., Cline T.L., Aptekar’ R.L., Frederiks(2005), D.D., The Golenetskii Konus-Wind and S.V., Il’inskii Helicon-Coronas-F V.N., detection Pal’shingamma-ray V.D. of repeater the SGR giant 1806-20. gamma-ray astro-ph/0502541 flare from the soft Mazets E.P., Aptekar’ R.L., Cline T.L., Frederiksvon Kienlin D.D., A., Goldsten Pal’shin J.O., V.D. Golenetskii (2008) S.V., AGalaxy Hurley Giant (M31). K., Flare ApJ, from 680: a 545-549 Soft Gamma RepeaterMcGill in Pulsar the Group Andromeda (2014) McGill Onlinehttp://www.physics.mcgill.ca/ Magnetar pulsar/magnetar/main.html Catalog. [64] [62] [63] [59] [60] [61] [57] [58] [55] [56] [54] [52] [53] [50] [51] SGR/AXP - are they magnetars? [49] PoS(FRAPWS2016)045 G.S.Bisnovatyi-Kogan 17 Superheavy, neutron overabundant nuclei are stable at high den- Yes. Gennady, do you allow me to think of "magnetars" as of neutron stars with G, surrounded by low-mass accretion disks? What is the source of the fission material in the NS crust? 14 10 ≤ sities, because high Fermi energygets of into degenerate lower electrons densities, as prohibit a beta-decays.and result make of When these a this starquake nuclei matter or unstable another against instability, fission. the Free beta neutrons decays appear, increase leading Z to nuclear explosion. G.S. BISNOVATYI-KOGAN: Jim BEALL: G.S. BISNOVATYI-KOGAN: SGR/AXP - are they magnetars? DISCUSSION Wolfgang KUNDT: surface B